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A terrestrial planet, telluric planet or rocky planet is a planet that is composed primarily of silicate rocks or metals. Within the Solar System, the terrestrial planets are the inner planets closest to the Sun. The terms "terrestrial planet" and "telluric planet" are derived from Latin words for Earth (Terra and Tellus), as these planets are, in terms of composition, "Earth-like".

Terrestrial planets have a solid planetary surface, making them substantially different from the usually larger gas giants, which are composed mostly of some combination of hydrogen, helium, and water existing in various physical states.


All terrestrial planets have approximately the same type of structure: a central metallic core, mostly iron, with a surrounding silicate mantle. The Moon is similar, but has a much smaller iron core. Io and Europa are also satellites that have internal structures similar to that of terrestrial planets. Terrestrial planets can have canyons, craters, mountains, volcanoes, and other surface structures, depending on the presence of water and tectonic activity. Terrestrial planets possess secondary atmospheres, generated through internal volcanism or comet impacts, in contrast to the gas giants, whose atmospheres are primary, captured directly from the original solar nebula.[1]

Solar terrestrial planetsEdit

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Earth's Solar System has four terrestrial planets: Mercury, Venus, Earth, and Mars. Only one terrestrial planet, Earth, is known to have an active hydrosphere.

During the formation of the Solar System, there were probably many more "terrestrial" planetesimals, but most merged with or were ejected by the four terrestrial planets.

Dwarf planets, like Ceres and Pluto, and other large asteroids are similar to terrestrial planets in the fact that they do have a solid surface, but are, on average, composed of more icy materials (Ceres and Pluto have a density of 2.1 g cm−3, and Haumea's density is similar to Pallas's 2.8 g cm−3).

Density trendsEdit

The uncompressed density of a terrestrial planet is the average density its materials would have at zero pressure. A greater uncompressed density indicates greater metal content. Uncompressed density differs from the true average density because compression within planet cores increases their density; the average density depends on planet size as well as composition.

Densities of the terrestrial planets
Object Density (g cm−3) Semi-major axis (AU)
Mean Uncompressed
Mercury 5.4 5.3 0.39
Venus 5.2 4.4 0.72
Earth 5.5 4.4 1.0
Mars 3.9 3.8 1.5

The density of terrestrial planets trends towards lower values as the distance from the Sun increases. The rocky minor planet Vesta orbiting outside of Mars is less dense than Mars still, at 3.4 g cm−3.

It is unknown whether extrasolar terrestrial planets in general will also follow this trend.

Extrasolar terrestrial planetsEdit

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Most of the planets found outside the Solar System are gas giants, because they are more easily detectable.[2][3][4] But since 2005, hundreds of potentially terrestrial extrasolar planets have been found, with several being confirmed as terrestrial. Most of these are super-Earths, i.e. planets with masses between Earth's and Neptune's; super-Earths may be gas planets or terrestrial, depending on their mass and other parameters.

During the early 1990s, the first extrasolar planets were discovered orbiting the pulsar PSR B1257+12, with masses of 0.02, 4.3, and 3.9 times that of Earth's, by pulsar timing.

When 51 Pegasi b, the first planet found around a star still undergoing fusion, was discovered, many astronomers assumed it to be a gigantic terrestrial,Template:Citation needed because it was assumed no gas giant could exist as close to its star (0.052 AU) as 51 Pegasi b did. It was later found to be a gas giant.

In 2005, the first planets around main-sequence stars that may be terrestrial were found: Gliese 876 d, has a mass 7 to 9 times that of Earth and an orbital period of just two Earth days. It orbits the red dwarf Gliese 876, 15 light years from Earth. OGLE-2005-BLG-390Lb, about 5.5 times the mass of Earth, orbits a star about 21,000 light years away in the constellation Scorpius. From 2007 to 2010, three (possibly four) potential terrestrial planets were found orbiting the red dwarf Gliese 581. The smallest, Gliese 581 e, is only about 1.9 Earth mass,[5] but orbits very close to the star. An ideal terrestrial planet would be 2 Earth masses with a 25-day orbital period around a red dwarf.[6] Two others, Gliese 581 c and Gliese 581 d, as well as a disputed planet, Gliese 581 g, are more-massive super-Earths orbiting in or close to the habitable zone of the star, so they could potentially be habitable, with Earth-like temperatures.

Another potentially habitable and terrestrial planet, HD 85512 b, was discovered in 2011; it has at least 3.6 times the mass of Earth.[7] But the radius and composition of all these planets are unknown.

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The first confirmed terrestrial exoplanet, Kepler-10b, was found in 2011 by the Kepler Mission, specifically designed to discover Earth-like planets around other stars using the transit method.[8]

In the same year, the Kepler Space Observatory Mission team released a list of 1235 extrasolar planet candidates, including six that are "Earth-size" or "super-Earth-size" (i.e. they have a radius less than 2 Earth radii)[9] and in the habitable zone.[10] Since then, Kepler has discovered hundreds of planets ranging from Moon-sized to super-Earths, with many more candidates in this size range (see image).

A number of other telescopes capable of directly imaging extrasolar terrestrial planets are also being designed. These include the Terrestrial Planet Finder, Space Interferometry Mission, Darwin, New Worlds Mission, and Overwhelmingly Large Telescope.

List of terrestrial exoplanetsEdit

The following exoplanets have a density of at least 5 g/cm3 and a mass below Neptune's and are thus very likely terrestrial:

Kepler-10b, Kepler-20b, Kepler-36b, Kepler-48b, Kepler-78b, Kepler-89b, Kepler-97b, Kepler-99b, Kepler-131b.

The Neptune-mass planet Kepler-10c also has a density >5 g/cm3 and is thus very likely terrestrial.


In 2013, astronomers reported, based on Kepler space mission data, that there could be as many as 40 billion Earth- and super-Earth-sized planets orbiting in the habitable zones of Sun-like stars and red dwarfs within the Milky Way Galaxy.[11][12][13] 11 billion of these estimated planets may be orbiting Sun-like stars.[14] The nearest such planet may be 12 light-years away, according to the scientists.[11][12] However, this does not give estimates for the number of extrasolar terrestrial planets, because there are planets as small as Earth that have been shown to be gas planets (see KOI-314c).[15]


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Several possible classifications for terrestrial planets have been proposed:[16]

Silicate planet
The standard type of terrestrial planet seen in the Solar System, made primarily of silicon-based rocky mantle with a metallic (iron) core.
Iron planet
A theoretical type of terrestrial planet that consists almost entirely of iron and therefore has a greater density and a smaller radius than other terrestrial planets of comparable mass. Mercury in the Solar System has a metallic core equal to 60–70% of its planetary mass. Iron planets are believed to form in the high-temperature regions close to a star, like Mercury, and if the protoplanetary disk is rich in iron.
Coreless planet
A theoretical type of terrestrial planet that consists of silicate rock but has no metallic core, i.e. the opposite of an iron planet. Although the Solar System contains no coreless planets, chondrite asteroids and meteorites are common in the Solar System. Coreless planets are believed to form farther from the star where volatile oxidizing material is more common.
Carbon planet (also called "diamond planet")
A theoretical class of planets, composed of a metal core surrounded by primarily carbon-based minerals. They may be considered a type of terrestrial planet if the metal content dominates. The Solar System contains no carbon planets, but does have carbonaceous asteroids.

See alsoEdit


  1. Dr. James Schombert (2004). Primary Atmospheres (Astronomy 121: Lecture 14 Terrestrial Planet Atmospheres). Department of Physics University of Oregon. Retrieved 22 December 2009.
  2. Carole Haswell, Transiting Exoplanets
  3. Michael Perryman, The Exoplanet Handbook
  4. Sara Seager, Exoplanets
  5. Lightest exoplanet yet discovered. ESO (ESO 15/09 - Science Release) (21 April 2009). Retrieved 15 July 2009.
  6. Template:Cite arXiv
  7. Template:Cite news
  9. Namely: KOI 326.01 [Rp=0.85], KOI 701.03 [Rp=1.73], KOI 268.01 [Rp=1.75], KOI 1026.01 [Rp=1.77], KOI 854.01 [Rp=1.91], KOI 70.03 [Rp=1.96] – Table 6). A more recent study found that one of these candidates (KOI 326.01) is in fact much larger and hotter than first reported. Grant, Andrew (8 March 2011). Exclusive: "Most Earth-Like" Exoplanet Gets Major Demotion—It Isn’t Habitable. 80beats. Discover Magazine. Retrieved 9 March 2011.
  10. Borucki, William J. (1 February 2011). Characteristics of planetary candidates observed by Kepler, II: Analysis of the first four months of data (PDF). arXiv. Retrieved 16 February 2011.
  11. 11.0 11.1 Template:Cite news
  12. 12.0 12.1 (31 October 2013)Prevalence of Earth-size planets orbiting Sun-like stars. Proceedings of the National Academy of Sciences of the United States of America.
  13. 17 Billion Earth-Size Alien Planets Inhabit Milky Way. (January 7, 2013). Retrieved January 8, 2013.
  14. Template:Cite news
  16. Naeye, Bob (24 September 2007). Scientists Model a Cornucopia of Earth-sized Planets. NASA, Goddard Space Flight Center. Retrieved 23 October 2013.

External linksEdit

Template:Solar System Template:Exoplanet Template:Extraterrestrial life

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